Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/32978
DC Field | Value | Language |
---|---|---|
dc.contributor.author | PEZZUTO, Stefano | en_US |
dc.contributor.author | ELIA, Davide Quintino | en_US |
dc.contributor.author | SCHISANO, EUGENIO | en_US |
dc.contributor.author | Strafella, F. | en_US |
dc.contributor.author | Di Francesco, J. | en_US |
dc.contributor.author | Sadavoy, S. | en_US |
dc.contributor.author | André, P. | en_US |
dc.contributor.author | BENEDETTINI, Milena | en_US |
dc.contributor.author | Bernard, J. P. | en_US |
dc.contributor.author | DI GIORGIO, Anna Maria | en_US |
dc.contributor.author | Facchini, A. | en_US |
dc.contributor.author | Hennemann, M. | en_US |
dc.contributor.author | Hill, T. | en_US |
dc.contributor.author | Könyves, V. | en_US |
dc.contributor.author | MOLINARI, Sergio | en_US |
dc.contributor.author | Motte, F. | en_US |
dc.contributor.author | Nguyen-Luong, Q. | en_US |
dc.contributor.author | Peretto, N. | en_US |
dc.contributor.author | Pestalozzi, M. | en_US |
dc.contributor.author | Polychroni, D. | en_US |
dc.contributor.author | RYGL, Kazi Lucie Jessica | en_US |
dc.contributor.author | Saraceno, P. | en_US |
dc.contributor.author | Schneider, N. | en_US |
dc.contributor.author | SPINOGLIO, Luigi Giuseppe Maria | en_US |
dc.contributor.author | TESTI, Leonardo | en_US |
dc.contributor.author | Ward-Thompson, D. | en_US |
dc.contributor.author | White, G. J. | en_US |
dc.date.accessioned | 2023-01-23T11:33:42Z | - |
dc.date.available | 2023-01-23T11:33:42Z | - |
dc.date.issued | 2012 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/32978 | - |
dc.description.abstract | We report far-infrared Herschel observations obtained between 70 μm and 500 μm of two star-forming dusty condensations, <ASTROBJ>[HKM99] B1-bS</ASTROBJ> and <ASTROBJ>[HKM99] B1-bN</ASTROBJ>, in the <ASTROBJ>B1</ASTROBJ> region of the Perseus star-forming cloud. In the western part of the Perseus cloud, <ASTROBJ>B1-bS</ASTROBJ> is the only source detected in all six PACS and SPIRE photometric bands, but it is not visible in the Spitzer map at 24 μm. B1-bN is clearly detected between 100 μm and 250 μm. We have fitted the spectral energy distributions of these sources to derive their physical properties, and find that a simple greybody model fails to reproduce the observed spectral energy distributions. At least a two-component model is required, consisting of a central source surrounded by a dusty envelope. The properties derived from the fit, however, suggest that the central source is not a Class 0 object. We then conclude that while B1-bS and B1-bN appear to be more evolved than a pre-stellar core, the best-fit models suggest that their central objects are younger than a Class 0 source. Hence, they may be good candidates to be examples of the first hydrostatic core phase. The projected distance between B1-bS and B1-bN is a few Jeans lengths. If their physical separation is close to this value, this pair would allow studying the mutual interactions between two forming stars at a very early stage of their evolution. <P />Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Appendices are available in electronic form at <A href="http://www.aanda.org">http://www.aanda.org</A> | en_US |
dc.language.iso | eng | en_US |
dc.title | Herschel observations of B1-bS and B1-bN: two first hydrostatic core candidates in the Perseus star-forming cloud | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201219501 | en_US |
dc.identifier.scopus | 2-s2.0-84867882870 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2012/11/aa19501-12/aa19501-12.html | en_US |
dc.identifier.url | http://arxiv.org/abs/1209.5290v1 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 547 | en_US |
dc.relation.firstpage | A54 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2012A&A...547A..54P | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | IRA Bologna | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.orcid | 0000-0001-7852-1971 | - |
crisitem.author.orcid | 0000-0002-9120-5890 | - |
crisitem.author.orcid | 0000-0003-1560-3958 | - |
crisitem.author.orcid | 0000-0002-3597-7263 | - |
crisitem.author.orcid | 0000-0002-4767-2360 | - |
crisitem.author.orcid | 0000-0002-9826-7525 | - |
crisitem.author.orcid | 0000-0003-4146-9043 | - |
crisitem.author.orcid | 0000-0001-8840-1551 | - |
crisitem.author.orcid | 0000-0003-1859-3070 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
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043FHSC.pdf | Pdf editoriale | 1.09 MB | Adobe PDF | View/Open |
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